A different procedure was followed for stars with Teff \(\le \)  8000 K. The widths of the Balmer lines are insensitive to changes in surface gravity for such sources ([1]}); spectral indicators for this kind of objects based on lines ratios are difficult to apply given their typically large values of \(v \sin i\) . Therefore, in these cases moved directly to the step where the pEWs are calculated in the observed spectrum and in the whole collection of models (Fig. REF ). Hence, the result of the \(\chi ^{2}\)  test yields a value of [M/H], but with a degeneracy in \(\log g\) . In fact, the three best models with \(\log g\) =3.5, 4.0, 4.5 fit the regions of the observed spectrum practically in the same way, hardly showing any variation in the pEWs of the regions explored. In order to find out which \(\log g\)  is closer to the stellar value, we have used an indirect method that consists of determining which of these \(\log g\)  is consistent with the distance from Gaia (E)DR3 [2]}, [3]}.
